Abstract
The critical equation in Prof. Einstein’s relativity theory of gravitation is given in the form (
du
/
dϕ
)
2
+
u
2
=
c
2
— 1/
h
2
+ 2
mu
/
h
2
+ 2
mu
3
, where
m
is the mass of the sun,
u
is the reciprocal of the distance of the moving body from the sun,
h
2
=
ma
(1—
e
2
),
c
2
— 1 = —
m
/
a
,
a
is the “major semi-axis of the orbit,” the units being astronomical, and
e
is the “excentricity” of the orbit. The foregoing equation can be integrated exactly, the functions involved being elliptic and not circular; and the approximations for the solar system are easily obtained, because the modulus of the elliptic functions is small.
Cited by
11 articles.
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